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Debris disks around main-sequence stars are believed to derive fromplanetesimal populations that have accreted at early epochs and survivedpossible planet formation processes. While debris disks must contain solids ina broad range of sizes - from big planetesimals down to tiny dust grains -debris disk observations are only sensitive to the dust end of the sizedistribution. Collisional models of debris disks are needed to "climb up" theladder of the collisional cascade, from dust towards parent bodies,representing the main mass reservoir of the disks. We have used our collisionalcode to generate five disks around a sun-like star, assuming planetesimal beltsat 3, 10, 30, 100, and 200 AU with 10 times the Edgeworth-Kuiper-belt massdensity, and to evolve them for 10 Gyr. Along with an appropriate scaling rule,this effectively yields a three-parametric set of reference disks (initialmass, location of planetesimal belt, age). For all the disks, we have generatedspectral energy distributions (SEDs), assuming homogeneous sphericalastrosilicate dust grains. A comparison between generated and actually observedSEDs yields estimates of planetesimal properties (location, total mass etc.).As a test and a first application of this approach, we have selected five disksaround sun-like stars with well-known SEDs. In four cases, we have reproducedthe data with a linear combination of two disks from the grid (an "asteroidbelt" at 3 AU and an outer "Kuiper belt"); in one case a single, outercomponent was sufficient. The outer components are compatible with "largeKuiper belts" of 0.2-50 earth masses (in the bodies up to 100 km in size) withradii of 100-200 AU.

Collisional and Thermal Emission Models of Debris Disks: Towards Planetesimal Population Properties